  Filamentary flows toward the centre of molecular clouds have been recognized
as a crucial process in the formation and evolution of stellar clusters. In
this paper, we present a comprehensive observational study that investigates
the gas properties and kinematics of the Giant Molecular Cloud G148.24+00.41
using the observations of CO (1-0) isotopologues. We find that the cloud is
massive (10$^5$ M$_\odot$) and is one of the most massive clouds of the outer
Galaxy. We identified six likely velocity coherent filaments in the cloud
having length, width, and mass in the range of 14$-$38 pc, 2.5$-$4.2 pc, and
(1.3$-$6.9) $\times$ 10$^3$ M$_\odot$, respectively. We find that the filaments
are converging towards the central area of the cloud, and the longitudinal
accretion flows along the filaments are in the range of $\sim$ 26$-$264
M$_\odot$ Myr$^{-1}$. The cloud has fragmented into 7 clumps having mass in the
range of $\sim$ 260$-$2100 M$_\odot$ and average size around $\sim$ 1.4 pc, out
of which the most massive clump is located at the hub of the filamentary
structures, near the geometric centre of the cloud. Three filaments are found
to be directly connected to the massive clump and transferring matter at a rate
of $\sim$ 675 M$_\odot$ Myr$^{-1}$. The clump hosts a near-infrared cluster.
Our results show that large-scale filamentary accretion flows towards the
central region of the collapsing cloud is an important mechanism for supplying
the matter necessary to form the central high-mass clump and subsequent stellar
cluster.
