  JWST has revealed a ubiquitous population of "little red dots" (LRDs) at
$z\gtrsim4$, selected via their red rest-frame optical emission and compact
morphologies. They are thought to be reddened by dust, whether in tori of
active galactic nuclei or the interstellar medium (ISM), though none have
direct dust detections to date. Informed by the average characteristics of 675
LRDs drawn from the literature, we provide ballpark constraints on the dust
characteristics of the LRD population and estimate they have average dust
masses of $\langle M_{dust}\rangle=(1.6^{+4.8}_{-0.9})\times10^{4}$ M$_\odot$,
luminosities of $\langle L_{IR}\rangle = (8^{+3}_{-5})\times10^{10}$ L$_\odot$
and temperatures of $\langle T_{dust}\rangle = 110^{+21}_{-36}$ K. Notably, the
spectral energy distributions are thought to peak at $\sim$100 K (rest-frame
20-30$\mu m$) regardless of heating mechanism, whether AGN or star formation.
Our predictions likely mean LRDs have, on average, submillimeter emission a
factor of $\sim$100$\times$ fainter than current ALMA limits provide. If one
assumes LRDs' rest-optical light is dominated by stars, the star-to-dust ratio
is a factor of $\sim$100$\times$ larger than expected from dust formation
models; this suggests LRDs' stellar masses may be significantly overestimated.
Despite their high apparent volume density, LRDs contribute negligibly (0.1%)
to the cosmic dust budget at $z\gtrsim4$ due to their low dust masses.
