  Type Ia supernovae originate from the explosion of carbon-oxygen white dwarfs
in binary systems, but the exact nature of their progenitors remains elusive.
The bulk properties of Type Ia supernova remnants, such as the radius and the
centroid energy of the Fe K$\alpha$ blend in the X-ray spectrum, are determined
by the properties of the supernova ejecta and the ambient medium. We model the
interaction between Chandrasekhar and sub-Chandrasekhar models for Type Ia
supernova ejecta and a range of uniform ambient medium densities in one
dimension up to an age of 5000 years. We generate synthetic X-ray spectra from
these supernova remnant models and compare their bulk properties at different
expansion ages with X-ray observations from \textit{Chandra} and
\textit{Suzaku}. We find that our models can successfully reproduce the bulk
properties of most observed remnants, suggesting that Type Ia SN progenitors do
not modify their surroundings significantly on scales of a few pc. Ambient
medium density and expansion age are the main contributors to the diversity of
the bulk properties in our models. Chandrasekhar and sub-Chandrasekhar
progenitors make similar predictions for the bulk remnant properties, but
detailed fits to X-ray spectra have the power to discriminate explosion
energetics and progenitor scenarios.
