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We report the first measurement of polarized thermal dust emission toward theentire early and massive Infrared Dark Cloud G11.11$-$0.12 taken by thepolarimeter SOFIA/HAWC+ at 214 $\mu m$ wavelength. Magnetic fields (B-fields)obtained from the polarized emission tend to be perpendicular to the filament'sspine. We produce a map of B-field strengths for the center region of thefilament. The strengths vary in the range of 100-600 $\mu\rm{G}$ and arestrongest along the filament's spine. The central region is sub-Alfv\'enic andmostly sub-critical meaning that B-fields dominate over turbulence and arestrong enough to resist gravitational collapse. The alignment and properties ofdust grains are studied in the filament using the RAdiative Torque (RAT)theory. We find the decrease of polarization degree $P$ with emission intensity$I$, i.e., depolarization effect, of the form $P\propto I^{-\alpha}$ with$\alpha\sim$0.8-0.9, implying a significant loss of grain alignment in thefilament's spine. The depolarization can be explained by the decrease in RATalignment efficiency toward the denser regions with lower dust temperature, andcannot be explained by the B-field tangling. We study the effect of theenhanced magnetic relaxation by embedded iron inclusions on RAT alignment andfind that the high polarization fraction $P\sim$20-30\% in the outer layer ofthe filament is potential evidence for the enhanced RAT alignment by magneticrelaxation. This is the first time this effect is evaluated in a filament.Based on the polarization fraction and RAT alignment theory, we find evidencefor grain growth in the filament.

B-fields And dust in interstelLar fiLAments using Dust POLarization (BALLAD-POL): I. The massive filament G11.11-0.12 observed by SOFIA/HAWC+