  We present a new measurement of structure growth at $z \simeq 0.08$ obtained
by correlating the cosmic microwave background (CMB) lensing potential map from
the \textit{Planck} satellite with the angular distribution of the 2MASS
Photometric Redshift galaxies. After testing for, and finding no evidence for
systematic effects, we calculate the angular auto- and cross-power spectra. We
combine these spectra to estimate the amplitude of structure growth using the
bias-independent $D_G$ estimator introduced by Giannantonio et al. 2016. We
find that the relative amplitude of $D_G$ with respect to the predictions based
on \textit{Planck} cosmology is $A_D(z=0.08) = 1.00 \pm 0.21$, fully consistent
with the expectations for the standard cosmological model. Considering
statistical errors only, we forecast that a joint analysis between an LSST-like
photometric galaxy sample and lensing maps from upcoming ground-based CMB
surveys like the Simons Observatory and CMB-S4 can yield sub-percent
constraints on the growth history and differentiate between different models of
cosmic acceleration.
