  The Cepheus Flare region consists of a group of dark cloud complexes that are
currently active in star formation. The aim of this work is to estimate the
motion of four clouds, L1147/1158, L1172/1174, L1228 and L1251 located at
relatively high Galactic latitude (b $\gt$ 14$^{\circ}$) in the Cepheus Flare
region. We study the relationship between the motion of the cloud with respect
to the magnetic field and the clump orientations with respect to both the
magnetic field and the motion. We estimated the motion of the molecular clouds
using the proper motion and the distance estimates of the young stellar objects
(YSOs) associated with them using the Gaia EDR3 data. By assuming that the YSOs
are associated with the clouds and share the same velocity, the projected
direction of motion of the clouds are estimated. We estimated a distance of
371$\pm$22 pc for L1228 and 340$\pm$ 7 pc for L1251 implying that all four
complexes are located at almost the same distance. Assuming that both the
clouds and YSOs are kinematically coupled, we estimated the projected direction
of motion of the clouds using the proper motions of the YSOs. All the clouds in
motion are making an offset of $\sim$ 30$^{\circ}$ with respect to the ambient
magnetic fields except in L1172/1174 where the offset is $\sim$ 45$^{\circ}$.
In L1147/1158, the starless clumps are found to be oriented predominantly
parallel to the magnetic fields while prestellar clumps show random
distribution. In L1172/1174, L1228 and L1251,the clumps are oriented randomly
with respect to magnetic field. With respect to the motion of the clouds, there
is a marginal trend that the starless clumps are oriented more parallel in
L1147/1158 and L1172/1174. In L1228, the clumps major axis are oriented more
randomly. In L1251, we find a bimodal trend in case of starless clumps.
