We present the results based on the optical R-band polarization observations of 280 stars distributed towards the dark globule LDN 1225. Gaia data release 2 parallaxes along with the polarization data of ∼200 stars have been used to (a) constrain the distance of LDN 1225 as 830±83 pc, (b) determine the contribution of interstellar polarization (ISP), and (c) characterize the dust properties and delineate the magnetic field (B-field) morphology of LDN 1225. We find that B-fields are more organized and exhibit a small dispersion of 12 • . Using the 12 CO molecular line data from the Purple Mountain Observatory (PMO), along with the column density, dispersion in B-fields, we estimate B-field strength to be ∼56 ± 10 µG, magnetic to turbulence pressure to be ∼3 ± 2, and the mass-to-magnetic flux ratio (in units of critical value) to be < 1. These results indicate the dominant role of B-fields in comparison to turbulence and gravity in rendering the cloud support. B-fields are aligned parallel to the low-density parts (traced by 12 CO map) of the cloud, in contrast they are neither parallel nor perpendicular to the high-density core structures (traced by 13 CO and C 18 O maps). LDN 1225 hosts two 70 µm sources which seem to be of low-mass Class 0 sources. The total-to-selective extinction derived using optical and near-infrared photometric data is found to be anomalous (R V = 3.4), suggesting dust grain growth in LDN 1225. Polarization efficiency of dust grains follows a power-law index of −0.7 inferring that optical polarimetry traces B-fields in the outer parts of the cloud.