  We report the first evidence for high-mass star formation triggered by
collisions of molecular clouds in M33. Using the Atacama Large
Millimeter/submillimeter Array, we spatially resolved filamentary structures of
giant molecular cloud 37 in M33 using $^{12}$CO($J$ = 2-1), $^{13}$CO($J$ =
2-1), and C$^{18}$O($J$ = 2-1) line emission at a spatial resolution of $\sim$2
pc. There are two individual molecular clouds with a systematic velocity
difference of $\sim$6 km s$^{-1}$. Three continuum sources representing up to
$\sim$10 high-mass stars with the spectral types of B0V-O7.5V are embedded
within the densest parts of molecular clouds bright in the C$^{18}$O($J$ = 2-1)
line emission. The two molecular clouds show a complementary spatial
distribution with a spatial displacement of $\sim$6.2 pc, and show a V-shaped
structure in the position-velocity diagram. These observational features traced
by CO and its isotopes are consistent with those in high-mass star-forming
regions created by cloud-cloud collisions in the Galactic and Magellanic Cloud
HII regions. Our new finding in M33 indicates that the cloud-cloud collision is
a promising process to trigger high-mass star formation in the Local Group.
