  We report a new, plasmoid-fed scenario for the formation of an eruptive
prominence (PF$^2$), involving reconnection and condensation. We use
grid-adaptive resistive two-and-a-half-dimensional magnetohydrodynamic (MHD)
simulations in a chromosphere-to-corona setup to resolve this plasmoid-fed
scenario. We study a pre-existing flux rope (FR) in the low corona that
suddenly erupts due to catastrophe, which also drives a fast shock above the
erupting FR. A current sheet (CS) forms underneath the erupting FR, with
chromospheric matter squeezed into it. The plasmoid instability occurs and
multiple magnetic islands appear in the CS once the Lundquist number reaches
$\sim 3.5\times 10^{4}$. The remnant chromospheric matter in the CS is then
transferred to the FR by these newly formed magnetic islands. The dense and
cool mass transported by the islands accumulates in the bottom of the FR,
thereby forming a prominence during the eruption phase. More coronal plasma
continuously condenses into the prominence due to the thermal instability as
the FR rises. Due to the fine structure brought in by the PF$^2$ process, the
model naturally forms filament threads, aligned above the polarity inversion
line. Synthetic views at our resolution of $15 \mathrm{km}$ show many details
that may be verified in future high-resolution observations.
