High-z galaxy protoclusters are the nurseries of young, rapidly growing star-forming galaxies, which, upon quenching, become the backbone of massive clusters at z<1. During the cosmic noon, these large-scale structures are fed by vigorous cold gas streams fueling the star formation activities of their members. At times, this star formation may be detectable in the rest-frame UV/optical, but during intense starbursts, it can be heavily obscured by dust, emitting mainly in the rest-frame infrared, only accessible to the game-changer JWST. Up to now, this has prevented us from obtaining an unambiguous view of the stellar mass growth, quenching propagation, and the impact of environmental effects on the internal distribution of gas/dust and star formation activities in protoclusters. We use rest-frame UV-to-NIR star-formation tracers, including Paschen-β narrow-band imaging from JWST/NIRCam, together with CO(1-0) molecular gas masses from ATCA, to discuss the relative importance of these processes in regulating the accelerated evolution of star-forming and starbursting galaxies in one of the most massive and best-studied systems at z>2: the Spiderweb protocluster.