  We present measurements of the dependence of the clustering amplitude of
galaxies on their star formation rate (SFR) and stellar mass ($M_*$) at $0.7 <
z < 1.5$ to assess the extent to which environment affects these properties.
While these relations are well determined in the local universe, they are much
more poorly known at earlier times. For this analysis we make use of the
near-IR HST WFC3 grism spectroscopic data in the five CANDELS fields obtained
as part of the 3D-HST survey. We make projected 2-point correlation function
measurements using $\sim$6,000 galaxies with accurate redshifts, $M_*$ and
H$\alpha$ luminosities. We find a strong dependence of clustering amplitude on
H$\alpha$ luminosity and thus SFR. However, at fixed $M_*$, the clustering
dependence on H$\alpha$ luminosity is largely eliminated. We model the
clustering of these galaxies within the Halo Occupation Distribution framework
using the conditional luminosity function model and the newly developed
conditional stellar mass and H$\alpha$ luminosity distribution model. These
show that galaxies with higher SFRs tend to live in higher mass haloes, but
this is largely driven by the relationship between SFR and $M_*$. Finally, we
show that the small residual correlation between clustering amplitude and
H$\alpha$ luminosity at fixed $M_*$ is likely being driven by a broadening of
the SFR-$M_*$ relationship for satellite galaxies.
