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Alma Cycle 3 observations showed strong absorption from diffuse molecular gasin 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 towardthe 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 inALMA Cy 4 toward J1713-3418, J1717-3341, J1733-3722 and J1744-3116. Strongmolecular absorption from disk gas at $|\rmv| \la 30$ \kms\ was detected in alldirections, and absorption from the 3 kpc arm was newly detected toward J1717and J1744. However, only the sightline toward J1744 is dominated by moleculargas overall and no other sightlines showed molecular absorption from gas deepinside the bulge. No molecular absorption was detected toward J1717 where H Iemission 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 andkinematics like that seen near the Sun and in the Milky Way disk generally. Wemeasured isotopologic ratios N(\hcop)/N(H$^{13}$CO\p) $> 51~(3\sigma)$ for thebulge gas toward J1744 and $58\pm9$ and $64\pm4$ for the disk gas toward J1717and J1744, respectively, all well above the value of 20-25 typical of thecentral molecular zone.} %conclusions heading (optional), leave it empty ifnecessary {The kinematics and chemistry of the bulge gas observed toward J1744more nearly resemble that of gas in the Milky Way disk than in the centralmolecular zone.}

ALMA observations of molecular absorption in four directions toward the Galactic bulge