  The Small Magellanic Cloud (SMC) is the closest low-metallicity galaxy to the
Milky Way where the dynamical state of molecular clouds can be analyzed. We
present a CO(2-1) survey at 9 pc resolution obtained with the APEX telescope in
an extensive region of the SMC and characterize the properties of the molecular
clouds. We study the dynamical state and stability of these clouds uniformly.
We identify 177 molecular clouds within the SMC by using CPROPS, of which 124
clouds are fully resolved with signal-to-noise ratio $>$ 5. The scaling
relationships show that the SMC clouds are (on average) less turbulent and less
luminous than their inner Milky Way counterparts of similar size by a factor of
2 and 3, respectively, while for a fixed linewidth, the SMC clouds are
over-luminous by a factor of 3.5. Using the virial masses, we derive a CO-to-H2
conversion factor for the SMC CO clouds of 10.5 M$_{\odot}(K km s^{-1}
pc^{2})^{-1}$, measured at 9 pc resolution. We also determine a dust-based
conversion factor of 28 M$_{\odot}(K km s^{-1} pc^{2})^{-1}$, obtained at 12 pc
resolution. We find that the SMC clouds appear to be in approximate
gravitational virial equilibrium. We find that the cumulative mass functions
based on both the luminous mass and the virial mass are steeper than
$\frac{dN}{dM} \propto M^{-2}$, suggesting that most of the molecular mass of
the SMC is contained in low-mass clouds.
