  Protoplanetary disks, which are the natural consequence of the gravitational
collapse of the dense molecular cloud cores, host the formation of the known
planetary systems in our universe. Substantial efforts have been dedicated to
investigating the properties of these disks in the more mature Class II stage,
either via numerical simulations of disk evolution from a limited range of
initial conditions or observations of their dust continuum and line emission
from specific molecular tracers. The results coming from these two standpoints
have been used to draw comparisons. However, few studies have investigated the
main limitations at work when measuring the embedded Class 0/I disk properties
from observations, especially in a statistical fashion. In this study, we
provide a first attempt to compare the accuracy of some critical disk
parameters in Class 0/I systems, as derived on real ALMA observational data,
with the corresponding physical parameters that can be directly defined by
theoreticians and modellers in numerical simulations. The approach we follow
here is to provide full post-processing of the numerical simulations and apply
it to the synthetic observations the same techniques used by observers to
derive the physical parameters. We performed 3D Monte Carlo radiative transfer
and mock interferometric observations of the disk populations formed in a
magnetohydrodynamic (MHD) simulation model of disk formation through the
collapse of massive clumps with the tools \textsc{Radmc-3d} and \textsc{Casa},
respectively, to obtain their synthetic observations. With these observations,
we re-employed the techniques commonly used in disk modelling from their
continuum emissions to infer the properties that would most likely be obtained
with real interferometers. We then demonstrated how these properties may vary
with respect to the gas kinematics analyses and dust continuum modelling.
