In agreement with previous work, we show that the presence of the short-lived radionuclide (SLR) ²⁶Al in the early solar system was unlikely (less than 2% a priori probability) to be the result of direct introduction of supernova (SN) ejecta into the gaseous disk during the Class II stage of protosolar evolution. We also show that Bondi-Hoyle accretion of any contaminated residual gas from the Sun's natal star cluster contributed negligible ²⁶Al to the primordial solar system. Our calculations are consistent with the absence of the oxygen isotopic signature expected with any late introduction of SN ejecta into the protoplanetary disk. Instead, the presence of ²⁶Al in the oldest solar system solids (calcium-aluminum-rich inclusions (CAIs)) and its apparent uniform distribution with the inferred canonical ²⁶Al/²⁷Al ratio of (4.5-5) × 10^–5 support the inheritance of ²⁶Al from the Sun's parent giant molecular cloud. We propose that this radionuclide originated in a prior generation of massive stars that formed in the same molecular cloud and contaminated that cloud by Wolf-Rayet winds. We calculated the Galactic distribution of ²⁶Al/²⁷Al ratios that arise from such contamination using the established embedded cluster mass and stellar initial mass functions, published nucleosynthetic yields from the winds of massive stars, and by assuming rapid and uniform mixing into the cloud. Although our model predicts that the majority of stellar systems contain no ²⁶Al from massive stars, and that the a priori probability that the ²⁶Al/²⁷Al ratio will reach or exceed the canonical solar system value is only ~6%, the maximum in the distribution of nonzero values is close to the canonical ²⁶Al/²⁷Al ratio. We find that the Sun most likely formed 4-5 million years (Myr) after the massive stars that were the source of ²⁶Al. Furthermore, our model can explain the initial solar system abundance of a second, co-occurring SLR, ⁴¹Ca, if ~5 × 10⁵ yr elapsed between ejection of the radionuclides and the formation of CAIs. The presence of a third radionuclide, ⁶⁰Fe, can be quantitatively explained if (1) the Sun formed immediately after the first SNe from the earlier generation of stars; (2) only 5% of SN ejecta was incorporated into the molecular cloud, or (3) the radionuclide originated in an even earlier generation of stars whose contributions to other radionuclides with a shorter half-life had completely decayed.