  We report ALMA observations of [CI]($^3P_1-^3P_0$), C$^{13}$O, and CO$^{18}$
($J=1-0$) toward the central region of a nearby Seyfert galaxy NGC 613. The
very high resolutions of $0.26"\times0.23"(=22\times20$ pc) for [CI] and
$0.42"\times0.35"(=36\times30$ pc) for C$^{13}$O, and CO$^{18}$ resolve the
circum-nuclear disk (CND) and star-forming ring. The distribution of [CI] in
the ring resembles that of the CO emission, although [CI] is prominent in the
CND. This can be caused by the low intensities of the CO isotopes due to the
low optical depths under the high temperature in the CND. We found that the
intensity ratios of [CI] to C$^{12}$O(3-2) ($R_{\rm CI/CO}$) and to
C$^{13}$O(1-0) ($R_{\rm CI/C^{13}O}$) are high at several positions around the
edge of the ring. The spectral profiles of CO lines mostly correspond each
other in the spots of the ring and high $R_{\rm CI/CO}$, but those of [CI] at
spots of high $R_{\rm CI/CO}$ are different from CO. These results indicate
that [CI] at the high $R_{\rm CI/CO}$ traces different gas from that traced by
the CO lines. The [CI] kinematics along the minor axis of NGC 613 could be
interpreted as a bubbly molecular outflow. The outflow rate of molecular gas is
higher than star formation rate in the CND. The flow could be mainly boosted by
the AGN through its radio jets.
