  We present KRATOS, a comprehensive suite of 28 open access pure N-body
simulations of isolated and interacting LMC-like galaxies, to study the
formation of substructures in their disc after the interaction with an SMC-mass
galaxy. The primary objective of this paper is to provide theoretical models
that help interpreting the formation of general structures of an LMC-like
galaxy under various tidal interaction scenarios. This is the first paper of a
series that will be dedicated to the analysis of this complex interaction.
Simulations are grouped in 11 sets of at most three configurations each
containing: (1) a control model of an isolated LMC-like galaxy; (2) a model
that contains the interaction with an SMC-mass galaxy, and; (3) the most
realistic configuration where both an SMC-mass and MW-mass galaxies may
interact with the LMC-like galaxy. In each simulation, we analyse the orbital
history between the three galaxies and examine the morphological and kinematic
features of the LMC-like disc galaxy throughout the interaction. This includes
investigating the disc scale height and velocity maps. When a bar develops, our
analysis involves characterising its strength, length, off-centeredness and
pattern speed. The diverse outcomes found in the KRATOS simulations, including
the presence of bars, warped discs, or various spiral arm shapes (along with
the high spatial, temporal, and mass resolution used), demonstrate their
capability to explore a range of LMC-like galaxy morphologies. Those directly
correspond to distinct disc kinematic maps, making them well-suited for a
first-order interpretation of the LMC's kinematic maps. From the simulations we
note that tidal interactions can: boost the disc scale height; both destroy and
create bars, and; naturally explain the off-center stellar bars. The bar length
and pattern speed of long-lived bars are not appreciably altered by the
interaction.
