  The relative importance of magnetic fields, turbulence, and gravity in the
early phases of star formation is still not well understood. We report the
first high-resolution dust polarization observations at 850 $\mu$m around the
most massive clump, located at the hub of the Giant Molecular Cloud
G148.24+00.41, using SCUBA-2/POL-2 at the James Clerk Maxwell Telescope. We
find that the degree of polarization decreases steadily towards the denser
portion of the cloud. Comparing the intensity gradients and local gravity with
the magnetic field orientations, we find that local gravity plays a dominant
role in driving the gas collapse as the magnetic field orientations and gravity
vectors seem to point towards the dense clumps. We also find evidence of
U-shaped magnetic field morphology towards a small-scale elongated structure
associated with the central clump, hinting at converging accretion flows
towards the clump. Our observation has resolved the massive clump into multiple
substructures. We study the magnetic field properties of two regions, central
clump (CC) and northeastern elongated structure (NES). Using the modified
Davis-Chandrasekhar Fermi method, we determine that the magnetic field
strengths of CC and NES are $\sim$24.0 $\pm$ 6.0 $\mu$G and 20.0 $\pm$ 5.0
$\mu$G, respectively. The mass-to-flux ratios are found to be magnetically
transcritical/supercritical, while the Alfv$\acute{\text{e}}$n Mach number
indicates a trans-Alfv$\acute{\text{e}}$nic state in both regions. These
results, along with Virial analysis, suggest that at the hub of G148.24+00.41,
gravitational energy has an edge over magnetic and kinetic energies.
