  We measure the color and stellar mass dependence of clustering in
spectroscopic galaxies at $0.6 < z < 0.65$ using data from the Baryon
Oscillation Spectroscopic Survey component of the Sloan Digital Sky Survey. We
greatly increase the statistical precision of our clustering measurements by
using the cross-correlation of 66,657 spectroscopic galaxies to a sample of 6.6
million fainter photometric galaxies. The clustering amplitude $w(R)$ is
measured as the ratio of the mean excess number of photometric galaxies found
within a specified radius annulus around a spectroscopic galaxy to that from a
random photometric galaxy distribution. We recover many of the familiar trends
at high signal-to-noise ratio. We find the ratio of the clustering amplitudes
of red and blue massive galaxies to be $w_\text{red}/w_\text{blue} = 1.92 \pm
0.11$ in our smallest annulus of 75-125 kpc. At our largest radii (2-4 Mpc), we
find $w_\text{red}/w_\text{blue} = 1.24 \pm 0.05$. Red galaxies therefore have
denser environments than their blue counterparts at $z \sim 0.625$, and this
effect increases with decreasing radius. Irrespective of color, we find that
$w(R)$ does not obey a simple power-law relation with radius, showing a dip
around 1 Mpc. Holding stellar mass fixed, we find a clear differentiation
between clustering in red and blue galaxies, showing that clustering is not
solely determined by stellar mass. Holding color fixed, we find that clustering
increases with stellar mass, especially for red galaxies at small scales (more
than a factor of 2 effect over 0.75 dex in stellar mass).
