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Of all the factors that influence star formation, magnetic fields are perhapsthe least well understood. The goal of this paper is to characterize the 3Dmagnetic field properties of nearby molecular clouds through various methods ofstatistically analysing maps of polarized dust emission. Our study focuses onnine clouds, with data taken from the Planck Sky Survey as well as data fromthe Balloon-borne Large Aperture Submillimeter Telescope for Polarimetryobservations of Vela C. We compare the distributions of polarization fraction($p$), dispersion in polarization angles ($\mathcal{S}$), and hydrogen columndensity ($N_{\rm H}$) for each of our targeted clouds. To broaden the scope ofour analysis, we compare the distributions of our clouds' polarizationobservables with measurements from synthetic polarization maps generated fromnumerical simulations. We also use the distribution of polarization fractionmeasurements to estimate the inclination angle of each cloud's cloud-scalemagnetic field. We obtain a range of inclination angles associated with ourclouds, varying from 16{\deg} to 69{\deg}. We establish inverse correlationsbetween $p$ and both $\mathcal{S}$ and $N_{\rm H}$ in almost every cloud, butwe are unable to establish a statistically robust $\mathcal{S}$ versus $N_{\rmH}$ trend. By comparing the results of these different statistical analysistechniques, we are able to propose a more comprehensive view of each cloud's 3Dmagnetic field properties. These detailed cloud analyses will be useful in thecontinued studies of cloud-scale magnetic fields and the ways in which theyaffect star formation within these molecular clouds.

Characterising the Magnetic Fields of Nearby Molecular Clouds using Submillimeter Polarization Observations