  We present Atacama Large Millimetre/Sub-Millimetre Array (ALMA) observations
of IRAS 19132+1035, a candidate jet-ISM interaction zone near the black hole
X-ray binary (BHXB) GRS 1915+105. With these ALMA observations (combining data
from the 12 m array and the Atacama Compact Array), we map the molecular line
emission across the IRAS 19132+1035 region. We detect emission from the
$^{12}$CO [$J=2-1$], $^{13}$CO [$\nu=0$, $J=2-1$], C$^{18}$O [$J=2-1$], ${\rm
H}_{2}{\rm CO}$ [$J=3_{0,3}-2_{0,2}$], ${\rm H}_{2}{\rm CO}$
[$J=3_{2,2}-2_{2,1}$], ${\rm H}_{2}{\rm CO}$ [$J=3_{2,1}-2_{2,0}$], SiO
[$\nu=0$, $J=5-4$], CH$_3$OH [$J=4_{2,2}-3_{1,2}$], and CS [$\nu=0$, $J=5-4$]
transitions. Given the morphological, spectral, and kinematic properties of
this molecular emission, we present several lines of evidence that support the
presence of a jet-ISM interaction at this site, including a jet-blown cavity in
the molecular gas. This compelling new evidence identifies this site as a
jet-ISM interaction zone, making GRS 1915$+$105 the third Galactic BHXB with at
least one conclusive jet-ISM interaction zone. However, we find that this
interaction occurs on much smaller scales than was postulated by previous work,
where the BHXB jet does not appear to be dominantly powering the entire IRAS
19132+1035 region. Using estimates of the ISM conditions in the region, we
utilize the detected cavity as a calorimeter to estimate the time-averaged
power carried in the GRS 1915+105 jets of
$(8.4^{+7.7}_{-8.1})\times10^{32}\,{\rm erg\,s}^{-1}$. Overall, our analysis
demonstrates that molecular lines are excellent diagnostic tools to identify
and probe jet-ISM interaction zones near Galactic BHXBs.
