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I will present ALMA observations of the H13CO+, C17O, and CO line emission from the protostellar system HH 212 at ∼24 au spatial resolution and compare them with those of the HCO+, SiO, and SO lines reported in the literature. We find that the CO emission traces four distinct regions: (1) an outer outflow shell, (2) a rotating wind region between the SiO and CO shells, (3) a shocked, wide-angle inner X-wind inside the SiO shell, and (4) the jet. The origin of the outer CO outflow shell could be associated with entrained envelope material or an extended disk wind. The rotating wind, which is shocked, is launched from a radius of 9–15 au, slightly beyond that of the previously detected SO shell, which marks the boundary where the wide-angle X-wind interacts with and shocks the disk wind. Additionally, SO is found to be mixed with CO emission within the thick and extended rotating wind region. The large-scale shocked CO wind coexists with SO emission near the upper portion of the inner shocked region, converging above the inner SiO knots. The CO jet is traced by a chain of knots with roughly equal spacing, exhibiting quasiperiodicity, as reported for other jets in the literature. Meanwhile, the H13CO+ and C17O lines trace the emission from the rotating envelope surrounding the outflow.