  We studied the cloud-cloud collision candidate G323.18+0.15 based on
signatures of induced filaments, clumps, and star formation. We used archival
molecular spectrum line data from the SEDIGISM $^{13}$CO($J$\,=\,2--1) survey,
from the Mopra southern Galactic plane CO survey, and infrared to radio data
from the GLIMPSE, MIPS, Hi-GAL, and SGPS surveys. Our new result shows that the
G323.18+0.15 complex is 3.55kpc away from us and consists of three cloud
components, G323.18a, G323.18b, and G323.18c. G323.18b shows a perfect U-shape
structure, which can be fully complemented by G323.18a, suggesting a collision
between G323.18a and the combined G323.18bc filamentary structure. One dense
compressed layer (filament) is formed at the bottom of G323.18b, where we
detect a greatly increased velocity dispersion. The bridge with an intermediate
velocity in a position-velocity diagram appears between G323.18a and G323.18b,
which corresponds to the compressed layer. G323.18a plus G323.18b as a whole
are probably not gravitationally bound. This indicates that high-mass star
formation in the compressed layer may have been caused by an accidental event.
The column density in the compressed layer of about $1.36 \times
10^{22}$cm$^{-2}$ and most of the dense clumps and high-mass stars are located
there. The average surface density of classI and classII young stellar objects
(YSOs) inside the G323.18+0.15 complex is much higher than the density in the
surroundings. The timescale of the collision between G323.18a and G323.18b is
$1.59$Myr. This is longer than the typical lifetime of classI YSOs and is
comparable to the lifetime of classII YSOs.
