  Resolved debris disk features (e.g., warps, offsets, edges and gaps,
azimuthal asymmetries, radially thickened rings, scale heights) contain
valuable information about the underlying planetary systems, such as the
posited planet's mass, semi-major axis, and other orbital parameters. Most
existing models assume a single planet is sculpting the disk feature, but
recent observations of mature planetary systems (e.g., by radial velocity
surveys or \textit{Kepler}) have revealed that many planets reside in
multi-planet systems. Here we investigate if/how planet properties inferred
from single-planet models are compromised when multiple planets reside in the
system. For each disk feature, we build a two-planet model that includes a
planet b with fixed parameters and a planet c with a full range of possible
parameters. We investigate these two-planet systems and summarize the
configurations for which assuming a single planet (i.e., planet b) leads to
significantly flawed inferences of that planet's properties. We find that
although disk features are usually primarily dominated by a single planet, when
using single-planet models we are at risk of misinterpreting planet properties
by orders of magnitude in extreme cases. Specifically, we are at high risk of
misinterpreting planet properties from disk warps; at moderate risk from disk
edges and gaps, radially thickened rings, and scale height features; and at low
risk from host star-disk center offsets and azimuthal asymmetries. We summarize
situations where we can infer the need to use a multi-planet model instead of a
single-planet one from disk morphology dissimilarities.
