  The Structure, Excitation, and Dynamics of the Inner Galactic InterStellar
Medium (SEDIGISM) survey has produced high (spatial and spectral) resolution
$^{13}$CO (2-1) maps of the Milky Way. It has allowed us to investigate the
molecular interstellar medium in the inner Galaxy at an unprecedented level of
detail and characterise it into molecular clouds. In a previous paper, we have
classified the SEDIGISM clouds into four morphologies. However, how the
properties of the clouds vary for these four morphologies is not well
understood. Here, we use the morphological classification of SEDIGISM clouds to
find connections between the cloud morphologies, their integrated properties,
and their location on scaling relation diagrams. We observe that ring-like
clouds show the most peculiar properties, having, on average, higher masses,
sizes, aspect ratios and velocity dispersions compared to other morphologies.
We speculate that this is related to the physical mechanisms that regulate
their formation and evolution, for example, turbulence from stellar feedback
can often results in the creation of bubble-like structures. We also see a
trend of morphology with virial parameter whereby ring-like, elongated, clumpy
and concentrated clouds have virial parameters in a decreasing order. Our
findings provide a foundation for a better understanding of the molecular cloud
behaviour based on their measurable properties.
