  We present a 3-D ideal MHD simulation of magnetospheric accretion onto a
non-rotating star. The accretion process unfolds with intricate 3-D structures
driven by various mechanisms. First, the disc develops filaments at the
magnetospheric truncation radius ($R_T$) due to magnetic interchange
instability. These filaments penetrate deep into the magnetosphere, form
multiple accretion columns, and eventually impact the star at $\sim$30$^o$ from
the poles at nearly the free-fall speed. Over 50% (90%) of accretion occurs on
just 5% (20%) of the stellar surface. Second, the disc region outside $R_T$
develops large-scale magnetically dominated bubbles, again due to magnetic
interchange instability. These bubbles orbit at a sub-Keplerian speed,
persisting for a few orbits while leading to asymmetric mass ejection. The disc
outflow is overall weak because of mostly closed field lines. Third,
magnetically-supported surface accretion regions appear above the disc,
resembling a magnetized disc threaded by net vertical fields, a departure from
traditional magnetospheric accretion models. Stellar fields are efficiently
transported into the disc region due to above instabilities, contrasting with
the ``X-wind'' model. The accretion rate onto the star remains relatively
steady with a 23% standard deviation. The periodogram reveals variability
occurring at around 0.2 times the Keplerian frequency at $R_T$, linked to the
large-scale magnetic bubbles. The ratio of the spin-up torque to
$\dot{M}(GM_*R_T)^{1/2}$ is around 0.8. Finally, after scaling the simulation,
we investigate planet migration in the inner protoplanetary disc. The disc
driven migration is slow in the MHD turbulent disc beyond $R_T$, while
aerodynamic drag plays a significant role in migration within $R_T$.
