  Aims: To reveal the morphology, chemical composition, kinematics and to
establish the main processes prevalent in the gas at the foot points of the
giant molecular loops (GMLs) in the Galactic center region
  Methods: Using the 22-m Mopra telescope, we mapped the M$-3.8+0.9$ molecular
cloud, placed at the foot points of a giant molecular loop, in 3-mm range
molecular lines. To derive the molecular hydrogen column density, we also
observed the $^{13}$CO $(2-1)$ line at 1 mm using the 12-m APEX telescope. From
the 3 mm observations 12 molecular species were detected, namely HCO$^+$, HCN,
H$^{13}$CN, HNC, SiO, CS, CH$_3$OH, N$_2$H$^+$, SO, HNCO, OCS, and HC$_3$N.
  Results: Maps revealing the morphology and kinematics of the M$-3.8+0.9$
molecular cloud in different molecules are presented. We identified six main
molecular complexes. We derive fractional abundances in 11 selected positions
of the different molecules assuming local thermodynamical equilibrium.
  Conclusions: Most of the fractional abundances derived for the M$-3.8+0.9$
molecular cloud are very similar over the whole cloud. However, the fractional
abundances of some molecules show significant difference with respect to those
measured in the central molecular zone (CMZ). The abundances of the shock
tracer SiO are very similar between the GMLs and the CMZ. The methanol emission
is the most abundant specie in the GMLs. This indicates that the gas is likely
affected by moderate $\sim $ 30 km s$^{-1}$ or even high velocity (50 km
s$^{-1}$) shocks, consistent with the line profile observed toward one of the
studied position. The origin of the shocks is likely related to the flow of the
gas throughout the GMLs towards the foot points.
