  We calculate crustal properties of neutron stars, namely, mass ($M_{\rm
crust}$), radius ($R_{\rm crust}$) and fraction of moment of inertia ($\Delta
I/I$) from parametrizations of hadronic relativistic mean-field (RMF) model
consistent with symmetric and asymmetric nuclear matter constraints, as well as
some stellar boundaries. We verify which one are also in agreement with
restrictions of $\Delta I/I \geqslant 1.4\%$ and $\Delta I/I \geqslant 7\%$
related to the glitching mechanism observed in pulsars, such as the Vela one.
The latter constraint explains the glitches phenomenon when entrainment effects
are taken into account. Our findings indicate that these parametrizations pass
in the glitching limit for a neutron star mass range of $M\leqslant
1.82M_\odot$ ($\Delta I/I \geqslant 1.4\%$), and $M\leqslant 1.16M_\odot$
($\Delta I/I \geqslant 7\%$). We also investigate the influence of nuclear
matter bulk parameters on crustal properties and find that symmetry energy is
the quantity that produces the higher variations on $M_{\rm crust}$, $R_{\rm
crust}$, and~$\Delta I/I$. Based on the results, we construct a particular RMF
parametrization able to satisfy $\Delta I/I \geqslant 7\%$ even at
$M=1.4M_\odot$, the mass value used to fit data from the softer component of
the Vela pulsar X-ray spectrum. The model also presents compatibility with
observational data from PSR J1614-2230, PSR J0348+0432, and MSP J0740+6620
pulsars, as well as, with data from the Neutron Star Interior Composition
Explorer (NICER) mission.
