  We present a study connecting the physical properties of protostellar
envelopes to the morphology of the envelope-scale magnetic field. We use the
ALMA polarization observations of 55 young prtostars at 0.87 mm on
$\sim400-3000$ au scales from the {\em B}-field Orion Protostellar Survey
(BOPS) to infer the envelope-scale magnetic field and both dust and gas
emission on comparable scales to measure the envelope properties. We find that
the protostellar envelopes with compact polarized dust emission tend to have
lower envelope masses, than the sources with more extended envelopes. We also
find that protostars showing hourglass-field morphologies tend to have lower
velocity dispersions in their envelopes, whereas systems with spiral-field
morphologies have higher velocity dispersion. Combining with the disk
properties taken from the Orion VLA/ALMA Nascent Disk and Multiplicity (VANDAM)
survey, we connect envelope properties to fragmentation. Our results suggest
that envelope mass may not correlate with fragmentation, whereas turbulence
appears to promote fragmentation. On the other hand, we find that fragmentation
is suppressed in systems with pinched magnetic fields, suggesting that the
magnetic field play a role on providing additional support against
gravitational collapse, and the formation of an hourglass-like field may
coincide with enhanced magnetic braking that removes angular momentum and
hinders the formation of embedded disks. Nevertheless, significant misalignment
between magnetic field and outflow axes tends to reduce magnetic braking,
leading to the formation of larger disks.
