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Using a sample of BzK-selected galaxies at z~2 identified from theCFHT/WIRCAM near-infrared survey of GOODS-North, we discuss the relationbetween star formation rate (SFR), specific star formation rate (SSFR), andstellar mass (M_{*}), and the clustering of galaxies as a function of theseparameters. For star-forming galaxies (sBzKs), the UV-based SFR, corrected forextinction, scales with the stellar mass as SFR ~ M_{*}^{alpha} with alpha =0.74+/-0.20 down to M_{*} ~ 10^{9} M_{solar}, indicating a weak dependence onthe stellar mass of the SSFR. We also measure the angular correlation functionand hence infer the correlation length for sBzK galaxies as a function ofM_{*}, SFR, and SSFR, as well as K-band apparent magnitude. We show thatpassive galaxies (pBzKs) are more strongly clustered than sBzK galaxies at agiven stellar mass, mirroring the color-density relation seen at lowerredshifts. We also find that the correlation length of sBzK galaxies rangesfrom 4 to 20 h^{-1}Mpc, being a strong function of M_{K}, M_{*}, and SFR. Onthe other hand, the clustering dependence on SSFR changes abruptly at 2x10^{-9}yr^{-1}, which is the typical value for "main sequence" star-forming galaxiesat z~2. We show that the correlation length reaches a minimum at thischaracteristic value, and is larger for galaxies with both smaller and largerSSFRs; a dichotomy that is only marginally implied from the predictions of thesemi-analytical models. Our results suggest that there are two types ofenvironmental effects at work at z~2. Stronger clustering for relativelyquiescent galaxies implies that the environment has started to play a role inquenching star formation. At the same time, stronger clustering for galaxieswith elevated SSFRs ("starbursts") might be attributed to an increasedefficiency for galaxy interactions and mergers in dense environments.

Clustering properties of BzK-selected galaxies in GOODS-N: environmental quenching and triggering of star formation at z ~ 2