  Far-infrared (FIR) dust polarimetry enables the study of interstellar
magnetic fields via tracing of the polarized emission from dust grains that are
partially aligned with the direction of the field. The advent of high quality
polarimetric data has permitted the use of statistical methods to extract both
the direction and magnitude of the magnetic field. In this work, the
Davis-Chandrasekhar-Fermi technique is used to make maps of the plane-of-sky
(POS) component of the magnetic field in the Orion Molecular Cloud (OMC-1) by
combining polarization maps at 53, 89, 154 and 214 \micron\ from HAWC+/SOFIA
with maps of density and velocity dispersion. In addition, maps of the local
dispersion of polarization angles are used in conjuction with Zeeman
measurements to estimate a map of the strength of the line-of-sight (LOS)
component of the field. Combining these maps, information about the
three-dimensional magnetic field configuration (integrated along the
line-of-sight) is inferred over the OMC-1 region. POS magnetic field strengths
of up to 2 mG are observed near the BN/KL object, while the OMC-1 bar shows
strengths of up to a few hundred $\mu$G. These estimates of the magnetic field
components are used to produce maps of the mass-to-magnetic flux ratio
($M/\Phi$) -- a metric for probing the conditions for star formation in
molecular clouds -- and determine regions of sub- and super-criticality in
OMC-1. Such maps can provide invaluable input and comparison to MHD simulations
of star formation processes in filamentary structures of molecular clouds.
