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We present ALMA Band 6 (nu=233GHz, lambda=1.3mm) continuum observationstowards 68 'normal' star-forming galaxies within two Coma-like progenitorstructures at z=2.10 and 2.47, from which ISM masses are derived, providing thelargest census of molecular gas mass in overdense environments at theseredshifts. Our sample comprises galaxies with a stellar mass range of1x10^9M_sun - 4x10^11M_sun with a mean M_*~6x10^10M_sun. Combining thesemeasurements with multiwavelength observations and SED modeling, wecharacterize the gas mass fraction and the star formation efficiency, and inferthe impact of the environment on galaxies' evolution. Most of our detectedgalaxies (~70%) have star formation efficiencies and gas fractions similar tothose found for coeval field galaxies and in agreement with the field scalingrelations. However, we do find that the proto-clusters contain an increasedfraction of massive, gas-poor galaxies, with low gas fractions (f_gas<6-10%)and red rest-frame ultraviolet/optical colors typical of post-starburst andpassive galaxies. The relatively high abundance of passive galaxies suggests anaccelerated evolution of massive galaxies in proto-cluster environments. Thelarge fraction of quenched galaxies in these overdense structures also impliesthat environmental quenching takes place during the early phases of clusterassembly, even before virialization. From our data, we derive a quenchingefficiency of E_q~0.45 and an upper limit on the quenching timescale ofT_q<1Gyr.

On the Gas Content, Star Formation Efficiency, and Environmental Quenching of Massive Galaxies in Proto-Clusters at z~2.0-2.5