  Obscuration in quasars may arise from steep viewing angles along the dusty
torus, or instead may represent a distinct phase of supermassive black hole
growth. We test these scenarios by probing the host dark matter halo
environments of $\sim 1.4$ million WISE-selected obscured and unobscured
quasars at $\langle z \rangle = 1.4$ using angular clustering measurements as
well as cross-correlation measurements of quasar positions with the
gravitational lensing of the cosmic microwave background (CMB). We interpret
these signals within a halo occupation distribution (HOD) framework to conclude
that obscured systems reside in more massive effective halos ($ \sim 10^{12.9}
h^{-1} M_{\odot}$) than their unobscured counterparts ($ \sim 10^{12.6} h^{-1}
M_{\odot}$), though we do not detect a difference in the satellite fraction. We
find excellent agreement between the clustering and lensing analyses and show
that this implies the observed difference is robust to uncertainties in the
obscured quasar redshift distribution, highlighting the power of combining
angular clustering and weak lensing measurements. This finding appears in
tension with models that ascribe obscuration exclusively to orientation of the
dusty torus along the line-of-sight, and instead may be consistent with the
notion that some obscured quasars are attenuated by galaxy-scale or
circumnuclear material during an evolutionary phase.
