  Solar prominences represent large-scale condensations suspended against
gravity within the solar atmosphere. The Rayleigh-Taylor (RT) instability is
proposed to be one of the important fundamental processes leading to the
generation of dynamics at many spatial and temporal scales within these
long-lived, cool, and dense structures amongst the solar corona. We run 2.5D
ideal magnetohydrodynamic (MHD) simulations with the open-source MPI-AMRVAC
code far into the nonlinear evolution of an RT instability perturbed at the
prominence-corona interface. Our simulation achieves a resolution down to $\sim
23$ km on a 2D $(x,y)$ domain of size 30 Mm $\times$ 30 Mm. We follow the
instability transitioning from a multi-mode linear perturbation to its
nonlinear, fully turbulent state. Over the succeeding $\sim 25$ minute period,
we perform a statistical analysis of the prominence at a cadence of $\sim
0.858$ s. We find the dominant guiding $B_z$ component induces coherent
structure formation predominantly in the vertical velocity $V_y$ component,
consistent with observations, demonstrating an anisotropic turbulence state
within our prominence. We find power-law scalings in the inertial range for the
velocity, magnetic, and temperature fields. The presence of intermittency is
evident from the probability density functions of the field fluctuations, which
depart from Gaussianity as we consider smaller and smaller scales. In exact
agreement, the higher-order structure functions quantify the multifractality,
in addition to different scale characteristics and behavior between the
longitudinal and transverse directions. Thus, the statistics remain consistent
with the conclusions from previous observational studies, enabling us to
directly relate the RT instability to the turbulent characteristics found
within quiescent prominence.
