  We measure and analyze galaxy clustering and the dependence on luminosity,
color, age, stellar mass and specific star formation rate using Baryon
Oscillation Spectroscopic Survey (BOSS) galaxies at $0.48<z<0.62$. We fit the
monopole and quadrupole moments of the two-point correlation function (2PCF)
and its projection on scales of $0.1$ -- $60.2h^{-1}$Mpc, after having split
the catalog in a variety of ways. We find that the clustering dependence is
consistent with previous well-established results showing the broad trends
expected: For example, that brighter, redder, older, more massive and quenched
galaxies are more strongly clustered. We also investigate the dependence on
additional parameters previously derived from stellar population synthesis
model fits to the spectra. We find that galaxy clustering depends on look-back
formation time at a low level, while it has little dependence on metallicity.
To understand the physics behind these trends, we fit the clustering with a
simulation-based emulator to simultaneously model cosmology and galaxy bias
using a Halo Occupation Distribution framework. After marginalizing parameters
determining the background cosmology, galaxy bias, and a scaling parameter to
decouple halo velocity field, we find that the growth rate of large scale
structure as determined by the redshift-space distortions is consistent with
previous analysis using the full sample, and we do not find evidence that
cosmological constraints depend systematically on galaxy selection. This
demonstrates that cosmological inference using small scale clustering
measurements is robust to changes in the catalog selection.
