We revisit the relation between magnetic-field strength ($B$) and gas density ($rho$) for contracting interstellar clouds and fragments (or, cores), which is central in observationally determining the dynamical importance of magnetic fields in cloud
evolution and star formation. Recently, it has been claimed that a relation $B propto rho^{2/3} $ is statistically preferred over $B propto rho^{1/2}$ in molecular clouds, when magnetic field detections and nondetections from Zeeman observations are combined. This finding has unique observational implications on cloud and core geometry: The relation $B propto rho^{2/3} $ can only be realized under spherical contraction. However, no indication of spherical geometry can be found for the objects used in the original statistical analysis of the $B-rho$ relation. We trace the origin of the inconsistency to simplifying assumptions in the statistical model used to arrive at the $Bpropto rho^{2/3}$ conclusion and to an underestimate of observational uncertainties in the determination of cloud and core densities. We show that, when these restrictive assumptions are relaxed, $B propto rho^{1/2}$ is the preferred relation for the (self-gravitating) molecular-cloud data, as theoretically predicted four decades ago.
