  The present study provides statistical information on the coronal magnetic
field and intensity properties of small-scale bright and faint loops in the
quiet Sun. We aim to quantitatively investigate the morphological and
topological properties of the coronal magnetic field in bright and faint
small-scale loops, with the former known as coronal bright points (CBPs). We
analyse 126 small-scale loops using quasi-temporal imaging and line-of-sight
magnetic field observations. We employ a recently developed automatic tool that
uses a linear magneto-hydro-static model to compute the magnetic field in the
solar atmosphere and automatically match individual magnetic field lines with
small-scale loops. For most of the loops, we automatically obtain an excellent
agreement of the magnetic field lines from the LMHS model and the loops seen in
AIA 193 A. One stand-out result is that the magnetic field is non-potential. We
obtain the typical ranges of loop heights, lengths, intensities, mean magnetic
field strength along the loops and at loop tops, and magnetic field strength at
loop footpoints. We find that loops below the classic chromospheric height of
1.5 Mm are flatter suggesting that non-magnetic forces (one of which is the
plasma pressure) play an important role below this height. We find a strong
correlation (Pearson coefficient of 0.9) between loop heights and lengths. The
average intensity along the loops correlates stronger with the average magnetic
field along the loops than with the field strength at loop tops. The latter
correlation indicates that the energy release in the loops is more likely
linked to the average magnetic field along the loops than the field strength on
the loop tops. In other words, the energy is probably released all along the
loops, but not just at the loop top. This result is consistent with the recent
benchmarking radiative 3D MHD model of N\'obrega-Siberio etal.
