  We test for galactic conformity at $0.2<z<1.0$ to a projected distance of 5
Mpc using spectroscopic redshifts from the PRism MUlti-object Survey (PRIMUS).
Our sample consists of $\sim60,000$ galaxies in five separate fields covering a
total of $\sim5.5$ square degrees, which allows us to account for cosmic
variance. We identify star-forming and quiescent "isolated primary" (i.e.,
central) galaxies using isolation criteria and cuts in specific star formation
rate. We match the redshift and stellar mass distributions of these samples, to
control for correlations between quiescent fraction and redshift and stellar
mass. We detect a significant $(>3\sigma)$ one-halo conformity signal, or an
excess of star-forming neighbors around star-forming central galaxies, of
$\sim5$% on scales of 0-1 Mpc and a $2.5\sigma$ two-halo signal of $\sim1$% on
scales of 1-3 Mpc. These signals are weaker than those detected in SDSS and are
consistent with galactic conformity being the result of large-scale tidal
fields and reflecting assembly bias. We also measure the star-forming fraction
of central galaxies at fixed stellar mass as a function of large-scale
environment and find that central galaxies are more likely to be quenched in
overdense environments, independent of stellar mass. However, we find that
environment does not affect the star formation efficiency of central galaxies,
as long as they are forming stars. We test for redshift and stellar mass
dependence of the conformity signal within our sample and show that large
volumes and multiple fields are required at intermediate redshift to adequately
account for cosmic variance.
