  Recently, a collision-induced magnetic reconnection (CMR) mechanism was
proposed to explain a dense filament formation in the Orion A giant molecular
cloud. A natural question is that whether CMR works elsewhere in the Galaxy. As
an initial attempt to answer the question, this paper investigates the
triggering of CMR and the production of dense gas in a flat-rotating disk with
a modified BiSymmetric Spiral (BSS) magnetic field. Cloud-cloud collisions at
field reversals in the disk are modeled with the Athena++ code. Under the
condition that is representative of the warm neutral medium, the cloud-cloud
collision successfully triggers CMR at different disk radii. However, dense gas
formation is hindered by the dominating thermal pressure, unless a moderately
stronger initial field $\gtrsim5\mu$G is present. The strong-field model,
having a larger Lundquist number $S_L$ and lower plasma $\beta$, activates the
plasmoid instability in the collision midplane, which is otherwise suppressed
by the disk rotation. We speculate that CMR can be common if more clouds
collide along field reversals. However, to witness the CMR process in numerical
simulations, we need to significantly resolve the collision midplane with a
spatial dynamic range $\gtrsim10^6$. If Milky Way spiral arms indeed coincide
with field reversals in BSS, it is possible that CMR creates or maintains dense
gas in the arms. High-resolution, high-sensitivity Zeeman/Faraday-Rotation
observations are crucial for finding CMR candidates that have helical fields.
