  Alma Cycle 3 observations showed strong absorption from diffuse molecular gas
in the bulge at -200 \kms\ $< {\rm v} < -140$ \kms\ toward J1744-3116 (l,b)=
(-2.13d,-1d) We aimed to test if bulge molecular gas could also be seen toward
the three other sufficiently strong mm-wave sources seen toward the bulgeat
$|b| < 3$\deg We took absorption profiles of \hcop (1-0) and other species in
ALMA Cy 4 toward J1713-3418, J1717-3341, J1733-3722 and J1744-3116. Strong
molecular absorption from disk gas at $|\rmv| \la 30$ \kms\ was detected in all
directions, and absorption from the 3 kpc arm was newly detected toward J1717
and J1744. However, only the sightline toward J1744 is dominated by molecular
gas overall and no other sightlines showed molecular absorption from gas deep
inside the bulge. No molecular absorption was detected toward J1717 where H I
emission from the bulge was previously known. As observed in \hcop, HCN, \cch\
and CS, the bulge gas toward J1744 at $v < -135$ \kms\ has chemistry and
kinematics like that seen near the Sun and in the Milky Way disk generally. We
measured isotopologic ratios N(\hcop)/N(H$^{13}$CO\p) $> 51~(3\sigma)$ for the
bulge gas toward J1744 and $58\pm9$ and $64\pm4$ for the disk gas toward J1717
and J1744, respectively, all well above the value of 20-25 typical of the
central molecular zone.} %conclusions heading (optional), leave it empty if
necessary {The kinematics and chemistry of the bulge gas observed toward J1744
more nearly resemble that of gas in the Milky Way disk than in the central
molecular zone.}
