  The rates at which mass accumulates into protostellar cores can now be
predicted in numerical simulations. Our purpose here is to develop methods to
compare the statistical properties of the predicted protostars with the
observable parameters. This requires (1) an evolutionary scheme to convert
numerically-derived mass accretion rates into evolutionary tracks and (2) a
technique to compare the tracks to the observed statistics of protostars. Here,
we use a 3D-Kolmogorov-Smirnov test to quantitatively compare model
evolutionary tracks and observations of Class0 protostars.
  We find that the wide range of accretion functions and timescales associated
with gravoturbulent simulations naturally overcome difficulties associated with
schemes that use a fixed accretion pattern. This implies that the location of a
protostar on an evolutionary track does not precisely determine the present age
or final accrued mass. Rather, we find that predictions of the final mass for
protostars from observed Tbol-Lbol values are uncertain by a factor of two and
that the bolometric temperature is not always a reliable measure of the
evolutionary stage. Furthermore, we constrain several parameters of the
evolutionary scheme and estimate a lifetime of Class0 sources of 2-6*10^4yrs,
which is related to the local free-fall time and thus to the local density at
the onset of the collapse. Models with Mach numbers smaller than six are found
to best explain the observational data. Generally, only a probability of 70%
was found that our models explain the current observations. This is caused by
not well understood selection effects in the observational sample and the
simplified assumptions in the models.
