HH 212 is a nearby (460 pc) protostellar jet discovered in H₂ powered by a Class 0 source, IRAS 05413-0104. We have mapped it in 850 μm continuum, SiO(J = 8-7), CO(J = 3-2), SO(N_J = 8₉-7₈), HCO⁺(J = 4-3), and H¹³CO⁺(J = 4-3) emission simultaneously at ~1'' resolution with the Submillimeter Array. Thermal dust emission is seen in continuum around the source, mainly arising from an inner envelope and a possible disk. The inner envelope is also seen with rotation in CO and HCO⁺, and probably in SO. Like H₂ emission, CO and SiO emission are seen along the jet axis but extending closer to the source, tracing the bow shocks and the continuous structures in between. SO emission is seen forming a jetlike structure extending from the source, likely tracing the jet near the launching region. The jet is episodic and bending. It may also be slightly precessing. A hint of jet rotation is also seen across the jet axis. Internal outflow shells are seen in CO and HCO⁺, associated with the bow shocks in the inner part of the jet. The bases of the HCO⁺ shells are seen with a hint of rotation, probably consisting mainly of the material extending from the inner envelope and even the possible disk. The bases of the outflow shells are also seen in H¹³CO⁺ and even the continuum, probably tracing the dense material extending from around the same regions.