function of stellar mass, and find good agreement with the observational results of @li06. Furthermore, we show that assuming central and satellite galaxies follow the same relation between stellar and halo mass, adding the clustering constraints does not tighten the constraints on our model parameters; i.e., any model that satisfies the mass function constraints will produce the correct clustering. Based on this result, we use our redshift-dependent CMF results to *predict* the clustering as a function of stellar mass and redshift. To date, observational measurements of clustering as a function of stellar mass have only been published for $z\lta 1$ [@meneux2008; @meneux2009]. We show that our model predictions agree very well with these measurements. Very soon it will be possible to test our predictions for redshifts beyond $z=1$ with the results from deep wide-field surveys (e.g. MUSYC, UKIDDS, etc). We again present convenient fitting functions for the galaxy bias as a function of both stellar mass and redshift. In a companion paper we will employ our estimates of galaxy bias in order to compute the “cosmic variance”, the uncertainty in observational estimates of the volume density of galaxies arising from the underlying large-scale density fluctuations.

This paper is organized as 