  We present DEEP2 galaxy clustering measurements at z~1 as a function of
stellar mass, star formation rate (SFR), and specific SFR (sSFR). We find a
strong positive correlation between stellar mass and clustering amplitude on
1-10 h^-1 Mpc scales for blue, star-forming galaxies with 9.5 < log(M_*/M_sun)
< 11 and no dependence for red, quiescent galaxies with 10.5 < log(M_*/M_sun) <
11.5. Using recently re-calibrated DEEP2 SFRs from restframe B-band magnitude
and optical colors, we find that within the blue galaxy population at z~1, the
clustering amplitude increases strongly with increasing SFR and decreasing
sSFR. For red galaxies there is no significant correlation between clustering
amplitude and either SFR or sSFR. Blue galaxies with high SFR or low sSFR are
as clustered on large scales as red galaxies. We find that the clustering trend
observed with SFR can be explained mostly, but not entirely, by the correlation
between stellar mass and clustering amplitude for blue galaxies. We also show
that galaxies above the star-forming "main sequence" are less clustered than
galaxies below the main sequence, at a given stellar mass. These results are
not consistent with the high sSFR population being dominated by major mergers.
We also measure the clustering amplitude of our samples on small scales (< 0.3
h^-1 Mpc) and find an enhanced clustering signal relative to the best-fit
large-scale power law for red galaxies with high stellar mass, blue galaxies
with high SFR, and both red and blue galaxies with high sSFR. The increased
small-scale clustering for galaxies with high sSFRs is likely linked to
triggered star formation in interacting galaxies. These measurements provide
strong constraints on galaxy evolution and halo occupation distribution models
at z~1.
