  The neutron star crustal EoS and transition point properties are computed
within a unified meta-modeling approach. A Bayesian approach is employed
including two types of filters: bulk nuclear properties are controlled from low
density effective field theory (EFT) predictions as well as the present
knowledge from nuclear experiments, while the surface energy is adjusted on
experimental nuclear masses. Considering these constraints, a quantitative
prediction of crustal properties can be reached with controlled confidence
intervals and increased precision with respect to previous calculations:
{$\approx 11\%$} dispersion on the crustal width and {$\approx 27\%$}
dispersion on the fractional moment of inertia. The crust moment of inertia is
also evaluated as a function of the neutron star mass, and predictions for mass
and radii are given for different pulsars. The possible crustal origin of Vela
pulsar glitches is discussed within the present estimations of crustal
entrainment, disfavoring a large entrainment phenomenon if the Vela mass is
above $1.4M_\odot$. Further refinement of the present predictions requires a
better estimation of the high order isovector empirical parameters, e.g.
$K_{sym}$ and $Q_{sym}$, and a better control of the surface properties of
extremely neutron rich nuclei.
