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Using a population of large-scale filaments extracted from an AREPOsimulation of a Milky Way-like galaxy, we seek to understand the extent towhich observed large-scale filament properties (with lengths $\gtrsim 100$ pc)can be explained by galactic dynamics alone. From an observer's perspective inthe disk of the galaxy, we identify filaments forming purely due to galacticdynamics, without the effects of feedback or local self-gravity. We find thatlarge-scale Galactic filaments are intrinsically rare, and we estimate that atmaximum approximately one filament per $\rm kpc^{2}$ should be identified inprojection, when viewed from the direction of our Sun in the Milky Way. In thisidealized scenario, we find filaments in both the arm and interarm regions, andhypothesize that the former may be due to gas compression in thespiral-potential wells, with the latter due to differential rotation. Using thesame analysis pipeline applied previously to observations, we analyze thephysical properties of large-scale Galactic filaments, and quantify theirsensitivity to projection effects and galactic environment (i.e. whether theylie in the arm or interarm regions). We find that observed "Giant MolecularFilaments" are consistent with being non-self-gravitating structures dominatedby galactic dynamics. Straighter, narrower, and denser "Bone-like" filaments,like the paradigmatic Nessie filament, have similar column densities, velocitygradients, and Galactic plane heights ($z\approx$ 0 pc) to those in our simplemodel, but additional physical effects (such as feedback and self-gravity) mustbe invoked to explain their lengths and widths.

Synthetic Large-Scale Galactic Filaments -- on their Formation, Physical Properties, and Resemblance to Observations