  We present the results of ALMA-ACA 7 m-array observations in
$^{12}$CO($J=2-1$), $^{13}$CO($J=2-1$), and C$^{18}$O($J=2-1$) line emission
toward the molecular-gas disk in the Local Group spiral galaxy M33 at an
angular resolution of 7".31 $\times$ 6".50 (30 pc $\times$ 26 pc). We combined
the ACA 7 m-array $^{12}$CO($J=2-1$) data with the IRAM 30 m data to compensate
for emission from diffuse molecular-gas components. The ACA+IRAM combined
$^{12}$CO($J=2-1$) map clearly depicts the cloud-scale molecular-gas structure
over the M33 disk. Based on the ACA+IRAM $^{12}$CO($J=2-1$) cube data, we
cataloged 848 molecular clouds with a mass range from $10^3$ $M_{\odot}$ to
$10^6$ $M_{\odot}$. We found that high-mass clouds ($\geq 10^5 M_{\odot}$) tend
to associate with the $8 \mu$m-bright sources in the spiral arm region, while
low-mass clouds ($< 10^5 M_{\odot}$) tend to be apart from such $8 \mu$m-bright
sources and to exist in the inter-arm region. We compared the cataloged clouds
with GMCs observed by the IRAM 30 m telescope at 49 pc resolution (IRAM GMC:
Corbelli et al. 2017), and found that a small IRAM GMC is likely to be
identified as a single molecular cloud even in ACA+IRAM CO data, while a large
IRAM GMC can be resolved into multiple ACA+IRAM clouds. The velocity dispersion
of a large IRAM GMC is mainly dominated by the line-of-sight velocity
difference between small clouds inside the GMC rather than the internal cloud
velocity broadening.
