The formation and evolution of the ultra-diffuse galaxies (UDGs) continue to remain a puzzle. Similarities and differences in the morphological and the kinematical properties of the UDGs with their possible precursors, namely low-surface brightness (LSB), L*-type high-surface brightness (HSB) and dwarf galaxies, may provide crucial constraints on their origin and evolution. To investigate the possible formation scenario of the UDGs, we selected samples of UDGs, LSBs, HSBs and dwarfs from the TNG50-1 sub-box of the IllustrisTNG simulation. We studied individual galaxy cutouts to evaluate the intrinsic shapes of their dark-matter (DM) and stellar components, orbital and kinematical properties related to their stellar velocity dispersion. Further, we constructed mock integral-field spectroscopic data using the SimSpin code to extract the stellar kinematic moment maps. We find that the isolated UDGs are prolate rotators similar to the dwarf population, while the tidally bound UDGs can exhibit both prolate- and oblate-rotating shapes. The DM and stellar velocity anisotropy properties of the UDGs suggest that they reside in a cored, dwarf-like halo and may be classified by early-type galaxies. Finally, the stellar kinematic properties suggest that both the UDGs and the dwarfs are slow-rotators having low to nearly no-rotations in contrast to the late-type, disc-dominated, fast-rotating LSBs and HSBs. Therefore, we may conclude that the UDGs and the dwarfs possibly have a common dynamical lineage.