The evolutionary instability dynamics, which is naturally excitable in an astrophysical complex gyrogravitating partially ionised molecular cloud in a magnetic field, is herein semianalytically investigated. It is rooted in a non-ideal classical non-relativistic magnetohydrodynamic (MHD) mean-fluidic model fabric. The effects of fluid kinematic viscosity, cosmic rays and tidal force field are concurrently included. Application of a standard normal mode analysis reduces the astrocloud into a unique generalised linear quartic dispersion relation having atypical variable coefficients. A numerical illustrative analysis shows that the instability is noticeably damped (grown) in the viscous (inviscid) domains. The magnetic field and rotation have stabilising influences against thenon-local self-gravity. In contrast, the cosmic ray pressure and tidal interaction destabilise the cloud along its self-gravity. We see that the ambipolar diffusion is the only non-ideal MHD factor with significant stimulus on themagneto-acoustic waves. The non-trivial results explored herematch with the prior predictions both as special cases and stimulating corollaries relevant in the bounded astrostructure creation dynamics.