We have developed a "pseudo-two-dimensional" model of solar flare loops from one-dimensional hydrodynamic calculations. The model consists of thermally isolated and fixed semicircular loops with different lengths and constant cross sections. To simulate a magnetic reconnection process, flare energy release is assumed to take place as heat depositions at the top portion of each loop, proceeding successively from the innermost loop to the outermost. In addition to temperature, density, and pressure distributions of the pseudo-two-dimensional flare loops, we compute surface brightness distributions of soft X-ray (SXR) emissions seen in bandpass filters of the Yohkoh Soft X-Ray Telescope (SXT). We find the following: (1) SXR brightening starts from the footpoints and expands into the upper corona as a result of chromospheric evaporation in the multiple-loop system. The resulting SXR-emitting structure has an apparent uniform width, which does not necessarily trace the underlying field lines. The outer edge of the structure corresponds to higher temperature regions (13-17 MK). (2) If the flare heating ceases before the structure is completely filled with evaporated plasma, a transient high-pressure region is produced at the top, which appears as a compact bright loop-top source in the SXT Be 119 μm filter, but not in the Al 0.1 μm filter.