  We performed a search of cloud-cloud collision (CCC) sites in the Sagittarius
A molecular cloud (SgrAMC) based on the survey observations using the Nobeyama
45-m telescope in the C$^{32}$S $J=1-0$ and SiO $v=0~J=2-1$ emission lines. We
found candidates being abundant in shocked molecular gas in the Galactic Center
Arc (GCA). One of them, M0.014-0.054, is located in the mapping area of our
previous ALMA mosaic observation. We explored the structure and kinematics of
M0.014-0.054 in the C$^{32}$S $J=2-1$, C$^{34}$S $J=2-1$, SiO $v=0~J=2-1$,
H$^{13}$CO$^+ J=1-0$, and SO $N,J=2,2-1,1$ emission lines and fainter emission
lines. M0.014-0.054 is likely formed by the CCC between the vertical molecular
filaments (VP) of the GCA, and other molecular filaments along Galactic
longitude. The bridging features between these colliding filaments on the PV
diagram are found, which are the characteristics expected in CCC sites. We also
found continuum compact objects in M0.014-0.054, which have no counterpart in
the H42$\alpha$ recombination line. They are detected in the SO emission line,
and would be "Hot Molecular Core (HMC)"s. Because the LTE mass of one HMC is
larger than the virial mass, it is bound gravitationally. This is also detected
in the CCS emission line. The embedded star would be too young to ionize the
surrounding molecular cloud. The VP is traced by poloidal magnetic field.
Because the strength of the magnetic field is estimated to be $\sim m$Gauss
using the CF method, the VP is supported against fragmentation. The star
formation in the HMC of M0.014-0.054 is likely induced by the CCC between the
stable filaments, which may be a common mechanism in the SgrAMC.
