  Using high-resolution observations from the 1.6 m New Solar Telescope (NST)
operating at the Big Bear Solar Observatory (BBSO), we report direct evidence
of merging/reconnection of cool H$\alpha$ loops in the chromosphere during two
homologous flares (B- and C-class) caused by a shear motion at the footpoint of
two loops. The reconnection between these loops caused the formation of an
unstable flux rope which showed counterclockwise rotation. The flux rope could
not reach the height of torus instability and failed to form a coronal mass
ejection. The HMI magnetograms revealed rotation of the negative/positive
(N1/P2) polarity sunspots in the opposite directions, which increased the right
and left-handed twist in the magnetic structures rooted at N1/P2. Rapid
photospheric flux cancellation (duration$\sim$20-30 min,
rate$\approx$3.44$\times$10$^{20}$ Mx h$^{-1}$) was observed during and even
after the first B6.0 flare and continued until the end of the second C2.3
flare. The RHESSI X-ray sources were located at the site of the loop's
coalescence. To the best of our knowledge, such a clear interaction of
chromospheric loops along with rapid flux cancellation has not been reported
before. These high-resolution observations suggest the formation of a small
flux rope by a series of magnetic reconnection within chromospheric loops
associated with very rapid flux cancellation.
