number counts, clustering and luminosity function of galaxies at $z\sim 2$ selected using the BzK selection criteria. The pBzK galaxies show a marked flattening in their number counts which cannot be explained by the effects of incompleteness, and a possible turn over at faint magnitudes. We conclude that, at this epoch, it is generally luminous, massive galaxies that are undergoing passive evolution. This is consistent with the down-sizing scenario, in which the most massive galaxies are formed first and are the first to evolve onto the red sequence [@Kodama_etal:2004].

The angular clustering of the passive galaxy sample is very strong, approximately $4$ times the amplitude of the sBzK population. This is in part due to their relatively narrow redshift distribution (K06), but a large difference remains after de-projection to the real-space correlation length. We find $r_0 = 15.0^{+1.9}_{-2.2}h^{-1}$Mpc and $r_0 = 6.75^{+0.34}_{-0.37}h^{-1}$Mpc for the pBzK and sBzK galaxies respectively. Our value for the correlation length of sBzKs is almost twice that found by [@Hayashi_etal:2007], who used a sample with similar limiting magnitude but with smaller field size ($180$ arcmin$^2$, compared with $\sim 2250$ arcmin$^2$ for the UDS). Our sample consists of more than 10 times the number of sBzKs than 